1996/04/12 by B. M. Poggianti, Poggianti, B. M., G. Barbaro +1 · 2 citations
Physics and Astronomy · #Astronomy #Astronomy and Astrophysical Research #Astrophysics #Astrophysics (astro-ph) #FOS: Physical sciences #Galactic corona #Galactic halo #Galaxies: Formation, Evolution, Phenomena #Galaxy #Halo #Physics #Redshift #Spiral galaxy #Star cluster #Star formation #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/9604066
published in University of Groningen research database (University of Groningen / Centre for Information Technology) 314(2), 379-392 (University of Groningen) · 15 pages, accepted for publication in Astronomy & Astrophysics, Latex version using l-aa style macro, preprint with figures available on request to: [email protected]
arxiv created 1996/04/12 · openalex publication_date 1996/04/12 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
In order to explain the spectroscopic observations of most of the galaxies in intermediate redshift clusters, bursts of star formation superimposed to the traditional scenario of galactic evolution are needed. The analysis of spectral lines and colours by means of an evolutionary synthesis model, including both the stellar contribution and the emission of the ionized gas, allows in most of the cases the determination of the time elapsed since the end of the burst and the fraction of galactic mass involved in it. In the four clusters considered (AC103, AC114, AC118 at \rm z=0.31 and Cl1358+6245 at \rm z=0.33), the theoretical analysis demonstrates that the bursts affect substantial galactic mass fractions, typically 30 % or more. The observations can be equally well reproduced by either elliptical+burst models or by spiral+burst models in which the star formation is truncated at the end of the burst. A way to determine the galactic original type is suggested.